Multimessengers from Core-Collapse Supernovae: Multidimensionality as a Key to Bridge Theory and Observation
Figure 15
Distribution of internal energy (left panel) and abundances of the ejecta (O, Si, Fe from left to right, normalized to solar) when the nonspherical shock is propagating in the O-rich layers at around ~20000 km along the pole (~1.5 s after bounce). For this model, the input neutrino luminosity is set as . Note that Fe in the right panel is the sum of , , and (from [248]).
